Table 2.
Parameters used in CIGALE to model the SFH (upper rows), dust attenuation (middle rows), and dust emission (lower row).
| Model | Parameter | Value |
|---|---|---|
| (1) | (2) | (3) |
| SFH | Age (Myr) | 11 000, 12 000, 13 000 |
| τmain (Myr) | 1000, 3000, 5000, 7000, 9000 | |
| Agebq (Myr) | 20, 50, 100, 300 | |
| rSFR | 0, 0.25, 0.5, 0.75, 1, 1.5, 2, 5, 10 | |
| Dust attenuation | E(B − V)lines (mag) | 0.05, 0.10, 0.15, 0.20, 0.25, 0.30, 0.35, 0.40, |
| 0.45, 0.50, 0.55, 0.60, 0.65, 0.70, 0.75, 0.8 | ||
| E(B − V)factor | 0.25, 0.5, 0.75 | |
| UV bump wavelength (nm) | 217.5 | |
| UV bump width (nm) | 35.0 | |
| UV bump amplitude | 0.0, 1.5, 3.0 | |
| Δδ | −1.0, −0.9, −0.8, −0.7, −0.6, −0.5, −0.4, −0.3, −0.2, −0.1,0,0.1,0.2,0.3 | |
| Dust emission | α | 2.0 |
Notes. Meaning of the parameters: 1) SFH: Age – age of the main stellar population in the galaxy, in Myr; τmain – e-folding time of the main stellar population model, in Myr; Agebq – age of the burst/quench episode, in Myr; and rsfr – ratio of the SFR after/before Agebq, values higher than one correspond to an enhancement of the SFR, whereas values lower than one correspond to a decrease; 2) dust attenuation: E(B − V)lines – colour excess of the nebular line light for both the young and old populations; E(B − V)factor – reduction factor to apply on E(B − V)lines to compute E(B − V)s the stellar continuum attenuation. Both young and old populations are attenuated by E(B − V)s; UV bump wavelength – central wavelength of the UV bump in nm; UV bump width – width (FWHM) of the UV bump in nm; UV bump amplitude – amplitude of the UV bump. For the Milky Way: 3; Δδ – slope delta of the power law modifying the attenuation curve. 3) Dust emission module: α – α slope in the Dale et al. (2014) model.
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